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The primary and secondary masses of the binary black holes (BBH) reported byLIGO/Virgo are correlated with a narrow dispersion that appears to increase inproportion to mass. The mean binary mass ratio $1.45\pm0.07$ we show isconsistent with pairs drawn randomly from the mass distribution of black holesin our Galaxy. However, BBH masses are concentrated around $\simeq 30M_\odot$,whereas black holes in our Galaxy peak at $\simeq 10M_\odot$. This massdifference can be reconciled by gravitational lensing magnification whichallows distant events to be detected with typically $z\simeq 2$, so thewaveform is reduced in frequency by $1+z$, and hence the measured chirp massesappear 3 times larger than their intrinsic values. This redshift enhancementalso accounts for the dispersion of primary and secondary masses, both of whichshould increase as $1+z$, thereby appearing to scale with mass, in agreementwith the data. Thus the BBH component masses provide independent support forlensing, implying most high chirp mass events have intrinsic masses like thestellar mass black holes in our Galaxy, coalescing at $z>1$, with only two lowmass BBH detections, of $\simeq 10M_\odot$ as expected for unlensed events inthe local Universe, $z\simeq 0.1$. This lensing solution requires a rapidlydeclining BBH event rate below $z<1$, which together with the observed absenceof BBH spin suggests most events originate within young globular clusters at$z>1$, via efficient binary capture of stellar mass black holes with randomlyoriented spins.

A Distant Origin For Magnified LIGO/Virgo Black Holes Implied By Binary Component Masses